A summary of the radio observations is presented in Table REF .
We inspected the data for bad antennas, bad time stamps and data impacted by radio frequency interference.
The data were analyzed using the standard reduction methodologies [1]}.
After the initial steps of flux density and bandpass calibration, all corrupted data were removed using standard routines.
The bandpass calibrated data for wide-bandwith GMRT data, i.e., the 250–500 MHz band and 1050–1450 MHz band data were split into five 40 MHz (from 300–500 MHz) and eight 50 MHz (from 1050–1450 MHz) subbands respectively. Subsequently, each subband data was analyzed separately, similar to narrowband “classic" GMRT data.
Several cycles of phase-only self-calibration and imaging were performed and the calibration solutions were applied to the target data to correct for residual phase errors. To take care of the wide-field imaging at low GMRT frequencies, we performed faceting imaging.
Problematic bright sources in the field of view whose side lobes affected the area of the target were subtracted, a.k.a. peeled; this (direction-dependent) calibration step improved the dynamic range of images. The calibrated data for five 40 MHz 250–500 MHz band data and eight 50 MHz 1050–1450 MHz band data were joined to form full 200 MHz and 400 MHz, respectively, wide-bandwidth-calibrated visibility data sets. The combined wide-bandwidth-calibrated data (and similarly the narrowband-calibrated “classic" GMRT data) were imaged using the casa task tclean.
We used 3D imaging (gridder = `widefield'), two Taylor coefficients (nterms = 2, tt0 and tt1) and Briggs weighting (robust = 0.5) in task tclean. A final amplitude-and-phase self-calibration with solution interval equal to the length of observation was then carried out using the gaincal and applycal tasks in casa.
The two Stokes polarizations, RR and LL, were combined to obtain the final total intensity Stokes I image, and corrected for the GMRT primary beam response.
This provides images at center frequencies (tt0) and the corresponding in-band spectral index maps (tt1/tt0).
The amplitude errors are estimated to be within 5% or less for archival narrow-bandwidth and wide-bandwidth GMRT data.
Table REF  also provides image properties, including the restoring beams and root mean square (rms) noise levels at half-power points of the final images.
The uncertainty in the flux density measurements are estimated as
\(\left[(S_\nu \times f)^2 + (\textsc {rms})^2 \times N_{\rm beams}\right]^{0.5},\) 
